We use a set of observations of the NGC 5194 NGC 5195 interactive pair obtained as part of the HST proposal 10452 (PI: Steven Beckwith). The images have been processed by the HST ACS pipeline using CALACS version used 8.2.0 (13 aug 2013), which includes bias subtraction, dark current correction, flatfielding as well as pixel-based CTE correction.
The images have been aligned using the DrizzlePac task TweakReg to better than 0.1 pixel precision. Then the WCS information in the header of the FLC files was updated with the help of the tweakback task. See other examples to learn how to complete these tasks on your own.
We provide the aligned FLC files upon request to show how to perform the matching of the sky between two tiles, each composed of four ACS/WFC FLC images.
Step 3 in the astrodrizzling process measures, subtracts and/or equalizes the sky from each input images and records the subtracted value in the image header. DrizzlePac 2.0 provides four algorithms for sky computation. In this example we ran all of them and compare the results.
This method is similiar to the original "skysub" algorithm used in previous versions of astrodrizzle. We first create a list (imlist.dat) containing the names of the eight images to drizzle. The command that we use to drizzle the images looks like this :
>>> astrodrizzle.AstroDrizzle('@imlist.dat',\ # name of input file output='f555w_localmin',\ # name of output file driz_sep_bits='2048,256,64,32',\ driz_cr_corr=yes,\ final_bits='2048,256,64,32',\ final_wht_type='EXP',\ final_wcs=yes,\ final_kernel='gaussian',\ final_pixfrac=1.0,\ final_scale=0.049,\ # ACS/WFC native pixel size final_rot=0.0,\ # rotate drizzled product final_ra=202.5076,\ # arbitrary value to center image final_dec=47.2437,\ # arbitrary value to center image skysub=yes,\ # turn on sky subtraction skymethod='localmin') # parameter to define the sky subtraction method
The output image is given in units of electrons/second. Figure 2 (left) shows the output image with the 'localmin' sky matching method applied. A clear horizontal border is seen between the two tiles. In order to display the final drizzled images and compare results, a hyperbolic sine stretch has been used.
This method computes differences in sky values between images in common sky regions. In this case computed sky values will be relative to the sky computed in one of the input images whose sky value will be set to 0. This setting will “equalize” sky values between the images in large mosaics. For this test, we ran the same code except with the line skymethod= 'match' . Figure 2 shows this output image at the same linear stretch as with the 'localmin' case.
This method computes sky values for each chip/image extension in all input images, finds the minimum sky value, and then it subtracts the same minimum sky value from all chips in all images. For this test, we ran the same code except with the line skymethod= 'globalmin'. Figure 2 shows the result of this drizzle experiment at the same linear stretch and the transition between tiles has dissapeared.
This method finds a minimum “global” sky value in all input images and then uses the ‘match’ method to equalize sky values between images. For this test, we ran the same code except with the line skymethod= 'globalmin+match'. The final drizzled images is shown below.
The 'sky' function in the DrizzlePac package updates the MDRIZSKY keyword in the headers of the input files, and provides a final value in the drizzled product. The table below shows the sky values computed by AstroDrizzle for the output images in this example.
SKYMETHOD MDRIZSKY (electrons)
The 'sky' function in the DrizzlePac package provides four methods to match the sky between tiles. The 'localmin' method is recommended for images with sparse fields (few astronomical sources) and the 'match' algorithm is recommended for images with complicated backgrounds such as nebulae, and large host galaxies.